On the variation of relative intensity of V- and R-components of the Hα emission line and their radial velocity in the spectrum of X Persei.

The 1974 - 1980 observations of the behaviour of the relative intensity of V- and R-components of the Hα emission line and their radial velocity of the Be star X Persei have been reexamined with the new data obtained in 1981 - 1982. It has been found that the variations of V/R and v_r(V, R) occurs with the 3-year cycle. It is suggested that the variations of the relative intensity of V- and R-components are the result of overlapping of the sharp emission on the wide (700 - 800 km/s) emission from the envelope surrounding the Be star. It is proposed that the sharp emission is provided by the secondary component orbiting around the Be star, or by a gas stream flowing from the secondary to the primary component.